Magnetic field effect on the fine structure of convective motions in the solar atmosphere |
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| Authors: | R I Kostyk |
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| Institution: | 1. Main Astronomical Observatory, National Academy of Sciences of Ukraine, ul. Acad. Zabolotnogo 27, Kyiv, 03680, Ukraine
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| Abstract: | Statistical properties of solar granulation in an active region on the solar surface from the photosphere to the lower chromosphere are studied. We use the values of the velocity, intensity, and magnetic field that were obtained at different heights in the solar atmosphere according to the observation data on the VTT telescope at Observatorio del Teide, Tenerife. The changes in the line??s parameters (central depth of the line, halfwidth, equivalent width, and central depth shift) and convective velocity are presented as functions of the value of the magnetic field. We propose a 16-column model of solar granulation depending on the direction of motion of convective elements and on the sign of contrast at two heights??in the continuous spectrum and in the highest layer (h = 650 km). We found that the magnetic field impedes the change in the sign and motion direction of convective elements. |
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